Knowing the composition of Jupiter's atmosphere is crucial for constraining Jupiter's bulk metallicity and formation history. Yet, constraining Jupiter's atmospheric water abundance is challenging due to its potential nonuniform distribution. Here, we explicitly resolve the water hydrological cycle in Jupiter's midlatitudes using high-resolution simulations. Falling precipitation leads to a significant large-scale depletion of water vapor beneath the lifting condensation level. A nonuniform water vapor distribution emerges in the midlatitude simulation with a changing Coriolis parameter across latitudes and spatially uniform cooling and heating. Water abundance at the 7-bar level varies by up to a factor of ten across latitudes, from subsolar to supersolar values. We propose that nonlinear large-scale eddies and waves tend to drift air parcels across latitudes along constant potential vorticity (PV) surfaces, thereby sustaining latitudinal dependencies in water vapor and the interplay between water distribution and large-scale dynamics. Therefore, water distribution is influenced by the vertical structure of density stratification and changing Coriolis parameter across Jupiter's midlatitudes, as quantified by PV. Additionally, the water hydrological cycle amplifies the specific energy of air parcels through the latent heat effect, thereby slowing down vertical mixing with a latent heat flux. The horizontal gradient of water is expected to be more pronounced with a supersolar water abundance. We suggest that similar interplays between precipitating condensates, planetary rotation, and distribution of condensable species generally exist in the weather layer of fast-rotating giant planets. The ongoing Juno mission and future Uranus mission may further reveal the nonuniform distribution of condensed species and their interplay with large-scale dynamics. A nonuniform water vapor distribution emerges in the midlatitude simulation with a changing Coriolis parameter across latitudes and spatially uniform cooling and heating. Water abundance at the 7-bar level varies by up to a factor of ten across latitudes, from subsolar to supersolar values. We propose that nonlinear large-scale eddies and waves tend to drift air parcels across latitudes along constant potential vorticity (PV) surfaces, thereby sustaining latitudinal dependencies in water vapor and the interplay between water distribution and large-scale dynamics. III) How can we improve our understanding of chemical distributions in planetary atmospheres, especially those that matter to measuring metallicity? We will first present our findings from the numerical simulation and then provide explanations to address the listed questions. The Simulated Water Distribution We simulated the water vapor distribution in Jupiter’s midlatitudes using the nonhydrostatic model SNAP ( 26 , 38 , 39 ) in a Cartesian box with linearly varying Coriolis parameter across the latitude (called beta-plane approximation). The simulation domain spans 45,000 km in latitude (y-direction) and 60,000 km in longitude (x-direction). We convert the distances in x − and y − directions to equivalent longitude and latitude with the radius of Jupiter and local Coriolis parameter on the β plane (see Fig. 1 caption). Vertically, the domain extends from ∼ 87 bar ( − 240 km) at the lower boundary to ∼ 0.002 bar (100 km) at the top, with the reference height ( z 0 = 0 km) set at 1 bar. The spatial resolution is 150 km in both longitude and latitude (about 0 . 1 ° ) and 2 km in the vertical direction. The spatial resolution allows us to resolve the Rossby deformation radius and the scale height of water vapor. The initial water vapor abundance in the deep reservoir is assumed to be three times solar and horizontally uniform. We propose that nonlinear large-scale eddies and waves which can propagate within the stratified atmosphere with a changing Coriolis parameter across latitudes (called the β effect by meteorologists) sustain the nonuniform distribution of water vapor shown in Figs. 1 A and D , 3 A , and 4 A . In our simulations, the latitudinal gradient of water vapor initially forms from a large-scale convective mixing during the spin-up phase ( Movie S2 ). Subsequently, The definition of PV in the context of Jupiter’s atmosphere could be, [4] PV = ( 2 Ω + ∇ × u ) ⏟ absolute vorticity · ∇ θ v ρ ⏟ weighted stratification ≈ ( f + ζ ) 1 ρ ∂ θ v ∂ z = ( f + ζ ) θ v ρ g N 2 , where Ω is the angular velocity of the planet, f = 2 Ω sin ϕ = f 0 + β 0 y is the Coriolis parameter that increases in latitude ϕ , θ v is the virtual potential temperature that represents the potential density of the air parcel adjusted by isentropic expansion or compression (i.e., buoyancy), ζ = ( ∇ × u ) · z ^ is the vertical component of relative vorticity, g is the gravity. The approximation in Eq. 4 could represent more than 99% of total PV, while the rest only contributes to less than 1% ( SI Appendix , Fig. S6 ). We find the leading terms in Eq. 4 that govern the simulated PV structure in Figs. 3 and 4 are the Coriolis parameter f , which increases in latitude, and the stratification N 2 , which is set by precipitation and peaks near 7.5 bars ( Fig. 4 B ). The variations of the other quantities are generally more minor than the change of f and N 2 across the domain (see Fig. 4 caption for numbers). The meridional gradient of the Coriolis parameter (i.e., planetary vorticity), β 0 , is fixed as a constant for the β -plane simulation, β 0 = 2 Ω / a ≈ 4.92 × 10 − 12 m − 1 s − 1 , where a is Jupiter’s planetary radii. Hence, the Coriolis parameter, f , is linear in latitude and calculated by f = 2 Ω sin ϕ 0 + β 0 y , where ϕ 0 = 20 ° N is the southern boundary of the domain and y is the meridional distance from the southern boundary. We adopt reflecting and free-slip boundary conditions in the meridional and vertical directions, but periodic boundary conditions in the longitudinal direction.